Observations and instruments at Lomnický štít Observatory

Transcription

1 Observations and instruments at Lomnický štít Observatory M. Kozák, J. Ambróz, P. Gömöry, A. Kučera, J. Rybák S. Tomczyk, S. Sewell, P. Aumiller, R. Summers, L. Sutherland, A. Watt Astronomický ústav SAV, Tatranská Lomnica High Altitude Observatory, NCAR, Boulder (USA)

2 AISAS 1943 Skalnaté pleso Observatory 1962 Lomnický štít Observatory 1979 Stará Lesná Observatory Department of Interplanetary Matter Department of Solar Physics Stellar department

3 1957 First unmanned satellite A short history of Observatory 1961 First man in space 1969 Men on the Moon 1990 Hubble telescope 1995 SOHO 2006 Hinode CoMP 2011 First observations 1962 Second coronagraph Photoelectric method

4 D=19.5 cm, f ~ 3m, DSUN = 4cm diffraction limited from 530 nm to 1083 nm spatial resolution: 0.67 at 530nm, 0.82 at 656nm, 1.36 at 1083nm photoelectric pointing system Coronagraphs

5 Observations since 1962 Coronal index, observation of oscillations, coronal mass ejections Spectrograf: Designed for wavelenght nm; dispersion at nm, at nm

6 Spectro-polarimeter Most solar activity derives its energy from coronal magnetic fields. Corona is the source of the solar wind with its embedded magnetic fields Many critical question will stay hidden until we can reliably measure the properties of coronal magnetic fields

7 Coronal Multi-channel Polarimeter (CoMP) Calibration Polarizer Stage Light Trap Occulting Disk Collimating Lens Pre-Filter Wheel Filter/Polarimeter Re-Imaging Lens Detector CoMP Observes: - Stokes I,U,Q,V - Fe XII nm, He I nm nm bandpass, 2.8 R(sun) Full Field-of-View, 4.5 arcsec/pixel

8 CoMP-S filter CoMP-S Tunable filter advances in broadband polarizers and super achromatic waveplates offer the possibility for the CoMP-S Lyot filter to operate over a much wider wavelenght range than CoMP. Super- achromatic l/2 plates: APSAW by ASTROPRIBOR lnominal Polarizer material: VIS700BC4 ~ 70% transmission

9 CoMP-S filter Recent polychromatic modulators based on FLCs can operate over a wide wavelenght range with high polarimetric efficiency Theoretical efficiency of the Stokes polarimeter for the CoMP-S

10 CoMP-S CoMP-S has several advantages: New technologies: optics, electronic cameras, computers The ZEISS coronagraph fixed focus of the re-imaging part Technological knowledge already gathered with the CoMP Main new features: wavelength range: , VIS + IR : several CHROM + COR lines more sensitive, faster and larger detectors for both IR and VIS ranges

11 CoMP-S instrument Dome Main parts of instrument: interface unit: connection of CoMP to the ZEISS coronagraph filter unit: Lyott filter. 2 filter wheels with NB filters and polarization & calibration optics detector unit: beam division optics, two cameras cabling computers and data storage Server room

12 Mechanical parts of CoMP-S mechanical interface filter module camera module cabinet on pier

13 Lyot filter Exploded view of the CoMP filter/polarimeter

14 Lyot filter Diagram of optical components Exit polarizer - Wollaston polarizing beamsplitter allowing silmultaneous imaging in the line and continuum Each of calcite stages is in a wide field configuration and has corresponding Nematic Liquid Crystal Variable for tuning.

15 Camera module Camera module with visible and infrared detectors

16 Detectors PCO scientific CMOS detector: pixel size: 6.5 µm x 6.5 µm Image sensor: CIS2051 Resolution: 2560 x 2160 pixel Quantum efficiency: > 54 peak spectral range: 370 nm nm Camera frame rate: 2560x2160

17 CoMP-S instrument Block diagram of CoMP-S instruments

18 Other electronic devices One control computer in server room 24 TB RAID system Electronic pointing system include clouds detection Automatic motor control (diffuser, instrument rotation and objective lens controller)

19 Measurements Observed prominence, no processed image

20 Measurements Prominence in H alpha spectral line

21 Thank you for your attention

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